Determining the modal mineralogy and the chemical composition of planetary surfaces from near-infrared spectroscopy: example of basaltic regions of Mars

Details Determining the modal mineralogy and the chemical composition of planetary surfaces from near-infrared spectroscopy: example of basaltic regions of Mars Determining the modal mineralogy and the chemical composition of planetary surfaces from near-infrared spectroscopy: example of basaltic regions of Mars

Oct 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011epsc.conf..390p&link_type=abstract

EPSC-DPS Joint Meeting 2011, held 2-7 October 2011 in Nantes, France. http://meetings.copernicus.org/epsc-dps2011, p.390

Physics

Scientific paper

Although Near-InfraRed (NIR) spectroscopy has been extensively used in chemistry and physics for many decades, this technique has been applied to the qualitative and quantitative analysis of planetary surfaces only relatively recently. Deconvolving a NIR reflectance spectrum to mineral abundance in an unambiguous way is indeed difficult, because the spectra are complex nonlinear functions of several parameters such as grain size, abundance, and material opacity. Multiple scattering theories using optical constants of minerals can provide approximate solutions to the radiative transfer in a compact medium. The modal mineralogy of a dozen of basaltic regions of Mars is obtained by modeling the OMEGA/MEx NIR reflectance spectra with the Shkuratov radiative transfer model. Modal mineralogies are then converted to bulk chemistries by combining the chemistries of the spectral library end-members used in the best fit in proportion to their modeled abundances. In doing so, a quantitative comparison of the OMEGA-derived chemical composition with chemistries measured in situ, in Martian meteorites and by remote observations is presented and the implications for igneous trends are discussed.

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